This section describes how the [M/H] values were obtained from the comparison of the observed spectra with photospheric models, being \(v \sin i\)  and \(\log g\)  additional outcomes of the process. Synthetic Castelli-Kurucz spectra computed with the suite of codes atlas9 [1]} were used throughout. These models do not consider disk-to-star accretion, which can produce a continuum excess -and possible line veiling in the coldest sources- mainly at wavelengths shorter than studied in this work [2]}, [3]}, [4]}.
